In favor of a possible pollution scenario for the \(^7\) Li in GaSS 1-26 is the
fact that indigenous \(^7\) Li production via the [1]}
mechanism is expected to occur during hot-bottom burning conditions (HBB),
when the outer part of the burning H-shell is included in the envelope
convection. A key aspect of HBB is the existence of a lower mass limit for
it to occur, which depends on metallicity [2]}. The
minimum initial mass for HBB is M\(_{\rm ini}\)\(\ge \) 5 M\(_\odot \)  at solar
metallicity [3]}, which can decrease down to
3 M\(_\odot \)  for very metal-poor stars [4]}. The
latter is obviously not the case given the otherwise normal spectrum
displayed by GaSS 1-26. The faintness and negligible reddening place GaSS
1-26 at a great distance from us; its Gaia \(e\) DR3 parallax is affected by a
large error, but it seems safe to argue that a lower limit to the distance
is 10 kpc. At a galactic latitude \(-\) 10\(^{\circ }_{.}\) 6, it means a height
over the galactic plane of \(z\)\(\ge \) 1.9 kpc. It would be rather atypical to
find a young and massive M\(_{\rm ini}\)\(\ge \) 5 M\(_\odot \)  star at such a large
height above the Galactic plane.
